The Merging Systems Identification (MeSsI) Algorithm.
|
|
- Phillip Brice Jefferson
- 6 years ago
- Views:
Transcription
1 The Merging Systems Identification (MeSsI) Algorithm. July 10, 2016
2 Table of contents 1 Why searching merging galaxy clusters? 2 The MeSsI Algorithm Machine learning algorithm applied for identification of substructures. Application of the MeSsI Algorithm to spectroscopy catalogues 3 Future Work
3 1 Why searching merging galaxy clusters? 2 The MeSsI Algorithm Machine learning algorithm applied for identification of substructures. Application of the MeSsI Algorithm to spectroscopy catalogues 3 Future Work
4 δ Mpc Mpc α α
5 You can study dark matter particle properties (Markevitch et al. 2004). Offset between Dark-Matter and gas. The great velocity of the secondary cluster. The survivor of the secondary cluster. You can test your favourite cosmological model. Studying the probability of finding a Bullet-like cluster (Hayashi et al. 2006; Farrar y Rosen 2007; Forero-Romero et al. 2010;...). Study the ICM properties through hidrodynamical simulations (Springel & Farrar. 2005; Lage & Farrar 2014; Zhang et al. 2014;...).
6 1 Why searching merging galaxy clusters? 2 The MeSsI Algorithm Machine learning algorithm applied for identification of substructures. Application of the MeSsI Algorithm to spectroscopy catalogues 3 Future Work
7
8 Clusters identification. We construct a mock catalogue based on the results of the application of the SAM Model of Guo et al to the Millenium simulation.
9 Clusters identification. We construct a mock catalogue based on the results of the application of the SAM Model of Guo et al to the Millenium simulation. We Perform a friend-of-friend algorithm (Merchan & Zandivares 2002 ) to the mock catalog in order to identify the clusters.
10 Clusters identification. We construct a mock catalogue based on the results of the application of the SAM Model of Guo et al to the Millenium simulation. We Perform a friend-of-friend algorithm (Merchan & Zandivares 2002 ) to the mock catalog in order to identify the clusters. We assign each identified cluster with a fof-group in the simulation.
11 Study of the merger trees. Based on the subhalos merger trees, we construct the merger tree for every fof group in the simulation.
12 Dressler-Shectman test. Non gaussianity test. Color. Number of galaxies.
13 Study of the identified substructures. We ran a second stage of a random forest algorithm, applied to the galaxies.
14 Study of the identified substructures. We ran a second stage of a random forest algorithm, applied to the galaxies. In order to define substructures we identify clumps of galaxies based on their proximity, using a mixture of gaussians weighted by the probability of each galaxy of being part of a substructure, calculated with the RF.
15 Study of the identified substructures. We ran a second stage of a random forest algorithm, applied to the galaxies. In order to define substructures we identify clumps of galaxies based on their proximity, using a mixture of gaussians weighted by the probability of each galaxy of being part of a substructure, calculated with the RF. After the substructure identification, each one was related with the subhalo in the mock that have more galaxies in the group identified by mclust.
16 g i = v i+1 v i (1) Study of the identified substructures. We ran a second stage of a random forest algorithm, applied to the galaxies. In order to define substructures we identify clumps of galaxies based on their proximity, using a mixture of gaussians weighted by the probability of each galaxy of being part of a substructure, calculated with the RF. After the substructure identification, each one was related with the subhalo in the mock that have more galaxies in the group identified by mclust. After that, we estimate the velocity dispersion and the virial radius. R vir = σ = ω i = i(ngal i) π ngal(ngal 1) 2 ngal R 1 i>j ij ngal 1 π ω i g i ngal(ngal 1) i=1
17 Study of the identified substructures. We compare the center of the identified substructures with the centers of the associated subhalos, finding a good estimation.
18 Study of the identified substructures. We compare the center of the identified substructures with the centers of the associated subhalos, finding a good estimation. We compare the virial radius of the identified substructures with the virial radius of the subhalos, finding that we are overestimating the real values.
19 Study of the identified substructures. We compare the center of the identified substructures with the centers of the associated subhalos, finding a good estimation. We compare the virial radius of the identified substructures with the virial radius of the subhalos, finding that we are overestimating the real values. We compare the velocity dispersion of the identified substructures with the velocity dispersion of the associated subhalos, finding that our values are in good concordance with the real values.
20 Mock Clusters
21 Application of the MeSsI Algorithm to spectroscopy catalogues We find 12 Clusters with high probability of been in a merger in the SDSS DR7. We find 4 Clusters with high probability of been in a merger in the WINGS Clusters. We find 16 Clusters with high probability of been in a merger in the HECs Clusters.
22
23 1 Why searching merging galaxy clusters? 2 The MeSsI Algorithm Machine learning algorithm applied for identification of substructures. Application of the MeSsI Algorithm to spectroscopy catalogues 3 Future Work
24 Future Work Perform astrophysical test over our sample of colliding cluster candidates looking for impose some constraints on dark matter particle properties. Apply the detection method to more deep real catalogs. Reconstruct the 3d merger with the Bayesian techniques presented by Dawson et al Study the physical properties of the galaxies that belong to the identified coliding substructures.
25
Simulating non-linear structure formation in dark energy cosmologies
Simulating non-linear structure formation in dark energy cosmologies Volker Springel Distribution of WIMPS in the Galaxy Early Dark Energy Models (Margherita Grossi) Coupled Dark Energy (Marco Baldi) Fifth
More informationAstro 406 Lecture 25 Oct. 25, 2013
Astro 406 Lecture 25 Oct. 25, 2013 Announcements: PS 7 due now PS 8 due next Friday ASTR 401: draft due next Monday thanks to the Planetarium-goers alternate makeup activity posted soon Next semester:
More informationN-body Simulations. Initial conditions: What kind of Dark Matter? How much Dark Matter? Initial density fluctuations P(k) GRAVITY
N-body Simulations N-body Simulations N-body Simulations Initial conditions: What kind of Dark Matter? How much Dark Matter? Initial density fluctuations P(k) GRAVITY Final distribution of dark matter.
More informationImage credit: Jee et al. 2014, NASA, ESA
SnowCluster 2015 The return of the merging galaxy subclusters of ACT-CL J0102-4915, El Gordo? (arxiv:1412.1826) Karen Y. Ng Will Dawson, David Wittman, James Jee, Jack Hughes, Felipe Menanteau, Cristóbal
More informationThe mass of a halo. M. White
A&A 367, 27 32 (2001) DOI: 10.1051/0004-6361:20000357 c ESO 2001 Astronomy & Astrophysics The mass of a halo M. White Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA e-mail: mwhite@cfa.harvard.edu
More informationThe Formation and Evolution of Galaxy Clusters
IAU Joint Discussion # 10 Sydney, July, 2003 The Formation and Evolution of Galaxy Clusters Simon D.M. White Max Planck Institute for Astrophysics The WMAP of the whole CMB sky Bennett et al 2003 > 105
More informationThe effect of large scale environment on galaxy properties
The effect of large scale environment on galaxy properties Toulouse, June 2017 Iris Santiago-Bautista The LSS baryonic component is composed by substructures of gas and galaxies embedded in dark matter
More informationarxiv:astro-ph/ v1 27 Nov 2000
A&A manuscript no. (will be inserted by hand later) Your thesaurus codes are: 02 (3.13.18) - methods: N-body simulations ASTRONOMY AND ASTROPHYSICS The mass of a halo Martin White arxiv:astro-ph/0011495v1
More informationarxiv: v1 [astro-ph.co] 5 May 2017
Draft version May 8, 2017 Preprint typeset using L A TEX style emulateapj v. 01/23/15 PROPERTIES AND ORIGIN OF GALAXY VELOCITY BIAS IN THE ILLUSTRIS SIMULATION Jia-Ni Ye 1,2,Hong Guo 1,Zheng Zheng 3, Idit
More informationBullet Cluster: A Challenge to ΛCDM Cosmology
Bullet Cluster: A Challenge to ΛCDM Cosmology Eiichiro Komatsu (Texas Cosmology Center, UT Austin) Fundamental Physics and Large-scale Structure, Perimeter Institute April 29, 2010 1 This talk is based
More informationcluster scaling relations and mass definitions
cluster scaling relations and mass definitions Andrey Kravtsov Department of Astronomy & Astrophysics Kavli Institute for Cosmological Physics The University of Chicago Abell 85 SDSS Abell 85 SDSS/ Abell
More informationClusters of Galaxies Groups: Clusters poor rich Superclusters:
Clusters of Galaxies Galaxies are not randomly strewn throughout space. Instead the majority belong to groups and clusters of galaxies. In these structures, galaxies are bound gravitationally and orbit
More informationTHE BOLSHOI COSMOLOGICAL SIMULATIONS AND THEIR IMPLICATIONS
GALAXY FORMATION - Durham -18 July 2011 THE BOLSHOI COSMOLOGICAL SIMULATIONS AND THEIR IMPLICATIONS JOEL PRIMACK, UCSC ΛCDM Cosmological Parameters for Bolshoi and BigBolshoi Halo Mass Function is 10x
More informationCosmological Simulations: Successes & Tensions of ɅCDM
Cosmological Simulations: Successes & Tensions of ɅCDM Volker Springel Large scale predictions Small scale predictions Challenges for ɅCDM from non-linear structure formation PASCOS 2011 Conference Cambridge,
More informationSources of scatter in cluster mass-observable relations
Great Lakes Cosmology Workshop 8, Columbus OH June 2, 2007 Sources of scatter in cluster mass-observable relations Paul Ricker University of Illinois National Center for Supercomputing Applications With
More informationGALAXY GROUPS IN THE THIRD DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY
The Astrophysical Journal, 630:759 763, 2005 September 10 # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. GALAXY GROUPS IN THE THIRD DATA RELEASE OF THE SLOAN DIGITAL
More informationClusters of Galaxies Groups: Clusters poor rich Superclusters:
Clusters of Galaxies Galaxies are not randomly strewn throughout space. Instead the majority belong to groups and clusters of galaxies. In these structures, galaxies are bound gravitationally and orbit
More informationCurrent status of the ΛCDM structure formation model. Simon White Max Planck Institut für Astrophysik
Current status of the ΛCDM structure formation model Simon White Max Planck Institut für Astrophysik The idea that DM might be a neutral, weakly interacting particle took off around 1980, following a measurement
More informationGravitational Lensing of the Largest Scales
What is dark matter? Good question. How do we answer it? Gravitational lensing! Gravitational lensing is fantastic Why Clusters of Galaxies Because they are cool!! Studying empirical properties of dark
More information4. Structure of Dark Matter halos. Hence the halo mass, virial radius, and virial velocity are related by
6-4-10see http://www.strw.leidenuniv.nl/ franx/college/galaxies10 10-c04-1 6-4-10see http://www.strw.leidenuniv.nl/ franx/college/galaxies10 10-c04-2 4. Structure of Dark Matter halos Obviously, we cannot
More informationHIERARCHICAL MODELING OF THE RESOLVE SURVEY
HIERARCHICAL MODELING OF THE RESOLVE SURVEY Sheila Kannappan, UNC Chapel Hill Faculty Fellow for SAMSI ASTRO Charlie Bonfield, UNC Chapel Hill Graduate Fellow for SAMSI ASTRO with input from Katie Eckert,
More informationGalaxy clusters. Dept. of Physics of Complex Systems April 6, 2018
Galaxy clusters László Dobos Dept. of Physics of Complex Systems dobos@complex.elte.hu É 5.60 April 6, 2018 Satellite galaxies Large galaxies are surrounded by orbiting dwarfs approx. 14-16 satellites
More informationGalaxy Ecology. an Environmental Impact Assessment. Frank van den Bosch (MPIA)
Galaxy an Environmental Impact Assessment Frank van den Bosch (MPIA) in collaboration with Xiaohu Yang (SHAO), Houjun Mo (UMass), Simone Weinmann (Zürich) Anna Pasquali (MPIA), Daniel Aquino (MPIA) Heidelberg,
More informationThe Los Cabos Lectures
January 2009 The Los Cabos Lectures Dark Matter Halos: 2 Simon White Max Planck Institute for Astrophysics EPS statistics for the standard ΛCDM cosmology Millennium Simulation cosmology: Ωm = 0.25, ΩΛ
More informationBeyond the spherical dust collapse model
Beyond the spherical dust collapse model 1.5M 1.0M M=1.66 10 15 M 0.65M 0.4M 0.25M Evolution of radii of different mass shells in a simulated halo Yasushi Suto Department of Physics and RESCEU (Research
More information4. Structure of Dark Matter halos. Hence the halo mass, virial radius, and virial velocity are related by
13-4-12see http://www.strw.leidenuniv.nl/ franx/college/galaxies12 12-c04-1 13-4-12see http://www.strw.leidenuniv.nl/ franx/college/galaxies12 12-c04-2 4. Structure of Dark Matter halos Obviously, we cannot
More informationClusters and groups of galaxies: internal structure and dynamics
Clusters and groups of galaxies: internal structure and dynamics Strong constraints on cosmological theories and on the nature of dark matter can be obtained from the study of cluster masses, mass distribution,
More informationarxiv: v2 [astro-ph.co] 11 Feb 2011
Mon. Not. R. Astron. Soc. 000, 2 (20) Printed 3 June 208 (MN LATEX style file v2.2) Linking haloes to galaxies: how many halo properties are needed? arxiv:.2492v2 [astro-ph.co] Feb 20 Eyal Neistein,2,
More informationEFFECT OF MERGERS ON THE SIZE EVOLUTION OF EARLY-TYPE GALAXIES
EFFECT OF MERGERS ON THE SIZE EVOLUTION OF EARLY-TYPE GALAXIES CARLO NIPOTI BOLOGNA UNIVERSITY Getting a Grip on Galaxy Girths, Tokyo, February 2015 NGC 474(Credit: Duc Atlas3D) Dry and wet galaxy mergers
More informationDark Matter -- Astrophysical Evidences and Terrestrial Searches
SFB 443 Bosen workshop 2010 Dark Matter -- Astrophysical Evidences and Terrestrial Searches Klaus Eitel, Karlsruhe Institute of Technology, KCETA, IK KIT University of the State of Baden-Württemberg and
More informationThe galaxy population in cold and warm dark matter cosmologies
The galaxy population in cold and warm dark matter cosmologies Lan Wang National Astronomical Observatories, CAS Collaborators: Violeta Gonzalez-Perez, Lizhi Xie, Andrew Cooper, Carlos Frenk, Liang Gao,
More informationClusters of galaxies
Clusters of galaxies Most galaxies belong to some larger bound structure. Conventionally consider groups and clusters, with characteristic properties: Groups Clusters Core radius 250 h -1 kpc 250 h -1
More information2. What are the largest objects that could have formed so far? 3. How do the cosmological parameters influence structure formation?
Einführung in die beobachtungsorientierte Kosmologie I / Introduction to observational Cosmology I LMU WS 2009/10 Rene Fassbender, MPE Tel: 30000-3319, rfassben@mpe.mpg.de 1. Cosmological Principles, Newtonian
More informationTwo-halo Galactic Conformity as a Test of Assembly Bias
Two-halo Galactic Conformity as a Test of Assembly Bias Angela Berti UC San Diego GalFRESCA 2018 1 Galactic Conformity Correlation between star formation rates (SFRs) of central galaxies and their satellites/neighbors
More informationThe Caustic Technique An overview
The An overview Ana Laura Serra Torino, July 30, 2010 Why the mass of? Small scales assumption of dynamical equilibrium Mass distribution on intermediate scales (1 10 Mpc/h) Large scales small over densities
More informationIdentifying and Characterizing Star-Forming Stellar Clumps
Deep Learning Applied to Galaxy Evolution: Identifying and Characterizing Star-Forming Stellar Clumps Christoph Lee (UCSC) Joel Primack (UCSC), Marc Huertas-Company (Paris Observatory), Yicheng Guo (University
More informationConstraints on physics of gas and dark matter from cluster mergers. Maxim Markevitch (SAO)
Constraints on physics of gas and dark matter from cluster mergers Maxim Markevitch (SAO) November 2005 1E 0657 56 Chandra 0.5 Msec image 0.5 Mpc z=0.3 An overheated cluster From M T relation: T= 14 kev:
More informationIs there a hope of discovering new physics in the Euclid era? Francisco Prada Instituto de Física Teórica UAM-CSIC, Madrid IAA-CSIC, Granada
Is there a hope of discovering new physics in the Euclid era? Francisco Prada Instituto de Física Teórica UAM-CSIC, Madrid IAA-CSIC, Granada ESAC,&October&15 th,&2015 Our$view$of$the$distant$Universe:$
More informationClusters of galaxies and the large scale structure of the universe. Gastão B. Lima Neto IAG/USP
Clusters of galaxies and the large scale structure of the universe Gastão B. Lima Neto IAG/USP IWARA, Maresias 10/2009 Our story begins... William Herschel recognizes the clustering of nebulae and their
More informationarxiv:astro-ph/ v1 1 Nov 2006
Modeling Chandra X-ray observations of Galaxy Clusters using Cosmological Simulations arxiv:astro-ph/0611013v1 1 Nov 2006 Daisuke Nagai 1, Andrey V. Kravtsov 2, and Alexey Vikhlinin 3,4 1 Theoretical Astrophysics,
More informationGalaxy Ecology. an Environmental Impact Assessment. Frank van den Bosch (MPIA)
Galaxy an Environmental Impact Assessment Frank van den Bosch (MPIA) in collaboration with Xiaohu Yang (SHAO), Houjun Mo (UMass), Simone Weinmann (Zürich) Anna Pasquali (MPIA), Daniel Aquino (MPIA) Aspen,
More informationCTA as a γ-ray probe for dark matter structures: Searching for the smallest clumps & the largest clusters
CTA as a γ-ray probe for dark matter structures: Searching for the smallest clumps & the largest clusters Moritz Hütten (MPP Munich) for the CTA consortium "The extreme Universe viewed in very-highenergy
More informationarxiv: v2 [astro-ph.co] 28 Oct 2011
SUBMITTED TO APJ MARCH, 209 Preprint typeset using LATEX style emulateapj v. /0/09 THE ROCKSTAR PHASE-SPACE TEMPORAL HALO FINDER AND THE VELOCITY OFFSETS OF CLUSTER CORES PETER S. BEHROOZI, RISA H. WECHSLER,
More informationThe halo-galaxy connection KITP, May 2017` Assembly bias. Simon White Max Planck Institute for Astrophysics
The halo-galaxy connection KITP, May 2017` Assembly bias Simon White Max Planck Institute for Astrophysics Halo clustering depends on formation history Gao, Springel & White 2005 The 20% of halos with
More informationBaryon Census in Hydrodynamical Simulations of Galaxy Clusters
Baryon Census in Hydrodynamical Simulations of Galaxy Clusters Susana Planelles (Univ.Trieste-INAF) Collaborators: S.Borgani (Univ. Trieste-INAF), G.Murante (INAF Torino), L.Tornatore (Univ. Trieste),
More informationA Systematic Approach to Cluster Formation in the Early Universe - Observations, Simulations, and New Surveys
A Systematic Approach to Cluster Formation in the Early Universe - Observations, Simulations, and New Surveys Yi-Kuan Chiang Roderik Overzier Karl Gebhardt University of Texas at Austin 09/10/2012 From
More informationIntroduction to simulation databases with ADQL and Topcat
Introduction to simulation databases with ADQL and Topcat Kristin Riebe, GAVO July 05, 2016 Introduction Simulation databases like the Millennium Database or CosmoSim contain data sets from cosmological
More informationOrigin of Bi-modality
Origin of Bi-modality and Downsizing Avishai Dekel HU Jerusalem Galaxies and Structures Through Cosmic Times Venice, March 2006 Summary Q: z
More informationNon-Standard Cosmological Simulations
7 th SSG:17/01/2018 Non-Standard Cosmological Simulations Juhan Kim, Changbom Park, & Benjamin L Huillier, Sungwook E. Hong KIAS & KASI Cosmology in Problem The Concordance LCDM: The Dark Age of Cosmology!
More informationCosmology on small scales: Emulating galaxy clustering and galaxy-galaxy lensing into the deeply nonlinear regime
Cosmology on small scales: Emulating galaxy clustering and galaxy-galaxy lensing into the deeply nonlinear regime Ben Wibking Department of Astronomy Ohio State University with Andres Salcedo, David Weinberg,
More informationUri Keshet / CfA Impact of upcoming high-energy astrophysics experiments Workshop, KAVLI, October 2008
Uri Keshet / CfA Impact of upcoming high-energy astrophysics experiments Workshop, KAVLI, October 008 Impact of upcoming high-energy astrophysics experiments Workshop, KAVLI, October 008 Relaxed, cool
More informationWeak Gravitational Lensing
Weak Gravitational Lensing Sofia Sivertsson October 2006 1 General properties of weak lensing. Gravitational lensing is due to the fact that light bends in a gravitational field, in the same fashion as
More informationThe Dynamics of Merging Clusters: A Monte Carlo Solution Applied to the Bullet and Musket Ball Clusters
The Dynamics of Merging Clusters: A Monte Carlo Solution Applied to the Bullet and Musket Ball Clusters University of California, Davis, Physics Department 5 de setembro de 2013 Seminário do grupo de Extragaláctica
More informationThe Dark Matter - Galaxy Connection: HOD Estimation from Large Volume Hydrodynamical Simulations
The Dark Matter - Galaxy Connection: HOD Estimation from Large Volume Hydrodynamical Simulations J. CASADO GÓMEZ (UAM) R. DOMÍNGUEZ-TENREIRO J. OÑORBE (UCA/Irvine) F. MARTINEZ - SERRANO (UMH) A. KNEBE
More informationIdentifying Star-Forming Clumps in CANDELS Galaxies
Properties of Dark Matter Halos: Environment Density, Mass Loss, and Connection to Galaxy Size Deep Learning Applied to Galaxy Evolution: Identifying Star-Forming Clumps in CANDELS Galaxies Christoph Lee
More informationDirect empirical proof of dark matter?
Direct empirical proof of dark matter? Masaki Mori Reference: D. Clowe et al., astro-ph/0608407 J.W. Moffat, astro-ph/0608675 ICRR CANGAROO Group Internal Seminar, 05-OCT-2006 Bergstroem and Goobar, Cosmology
More informationProbabilistic photometric redshifts in the era of Petascale Astronomy
Probabilistic photometric redshifts in the era of Petascale Astronomy Matías Carrasco Kind NCSA/Department of Astronomy University of Illinois at Urbana-Champaign Tools for Astronomical Big Data March
More informationThe subhalo populations of ΛCDM dark haloes
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 2 February 2008 (MN LATEX style file v1.4) The subhalo populations of ΛCDM dark haloes L. Gao, 1 S. D. M. White 1, A. Jenkins 2, F. Stoehr 3, V. Springel
More informationContents. List of Participants
Table of Introduction List of Participants page xi xiii 1 Galaxy clusters as probes of cosmology and astrophysics August E. Evrard 1 1.1 Introduction 1 1.2 Clusters as Dark Matter Potential Wells 4 1.3
More informationA unified multi-wavelength model of galaxy formation. Carlton Baugh Institute for Computational Cosmology
A unified multi-wavelength model of galaxy formation Carlton Baugh Institute for Computational Cosmology M81 Angel Lopez Sanchez A unified multi-wavelength model of galaxy formation Lacey et al. 2015 arxiv:1509.08473
More informationThe Current Status of Too Big To Fail problem! based on Warm Dark Matter cosmology
The Current Status of Too Big To Fail problem! based on Warm Dark Matter cosmology 172th Astronomical Seminar Dec.3 2013 Chiba Lab.M2 Yusuke Komuro Key Word s Too Big To Fail TBTF Cold Dark Matter CDM
More informationClustering, Proximity, and Balrog
Clustering, Proximity, and Balrog Eric Suchyta CCAPP Summer Series 01 July 2014 1 Outline Brief introduction to galaxy clustering New software called Balrog, particularly as it relates to clustering What
More informationMergers and Mass Assembly of Dark Matter Halos & Galaxies
Mergers and Mass Assembly of Dark Matter Halos & Galaxies Chung-Pei Ma Onsi Fakhouri James McBride (UC Berkeley) Mike Boylan-Kolchin (MPA --> Southern UC) Claude-Andre Faucher-Giguere Dusan Keres (Harvard
More informationMeasuring galaxy environments with group finders: Methods & Consequences
Measuring galaxy environments with group finders: Methods & Consequences Diego STALDER Doc student INPE, São Jose dos Campos, Brazil & IAP Marina TREVISAN Postdoc, IAP Manuel DUARTE former IAP Doc student
More informationCristóbal Sifón, Nick Battaglia, Matthew Hasselfield, Felipe Menanteau, and the ACT collaboration, 2016, MNRAS, 461, 248
1 We present galaxy velocity dispersions and dynamical mass estimates for 44 galaxy clusters selected via the Sunyaev-Zel dovich (SZ) effect by the Atacama Cosmology Telescope. Dynamical masses for 18
More information1. INTRODUCTION. Received 2003 March 12; accepted 2003 May 28. Ann Arbor, MI Fermi National Accelerator Laboratory, P.O.
The Astrophysical Journal Supplement Series, 148:243 274, 2003 October # 2003. The American Astronomical Society. All rights reserved. Printed in U.S.A. E A MERGED CATALOG OF CLUSTERS OF GALAXIES FROM
More informationGalaxy formation in WMAP1andWMAP7 cosmologies
MNRAS 428, 1351 1365 (2013) doi:10.1093/mnras/sts115 Galaxy formation in WMAP1andWMAP7 cosmologies Qi Guo, 1,2,3 Simon White, 2 Raul E. Angulo, 2 Bruno Henriques, 2 Gerard Lemson, 2 Michael Boylan-Kolchin,
More informationDARC - DYNAMICAL ANALYSIS OF RADIO CLUSTERS
DARC - DYNAMICAL ANALYSIS OF RADIO CLUSTERS Marisa Girardi, Rafael Barrena, and Walter Boschin (1) Dip. di Fisica, Univ. di Trieste Trieste Italy; (2) I.A.C.; (3) INAF-TNG Abstract Extended, diffuse radio
More informationASTRON 449: Stellar (Galactic) Dynamics. Fall 2014
ASTRON 449: Stellar (Galactic) Dynamics Fall 2014 In this course, we will cover the basic phenomenology of galaxies (including dark matter halos, stars clusters, nuclear black holes) theoretical tools
More informationarxiv: v2 [astro-ph.ga] 20 Mar 2015
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 24 March 2015 (MN LATEX style file v2.2) arxiv:1502.01339v2 [astro-ph.ga] 20 Mar 2015 The merger rate of galaxies in the Illustris Simulation: a comparison
More informationThe edge of darkness, and other halo surprises
The edge of darkness, and other halo surprises Benedikt Diemer ITC Fellow, Harvard-Smithsonian Center for Astrophysics (in collaboration with Andrey Kravtsov and Surhud More) APEC Seminar IPMU 4/7/26 Strength
More informationModelling the galaxy population
Modelling the galaxy population Simon White Max Planck Institut für Astrophysik IAU 277 Ouagadougou 1 The standard model reproduces -- the linear initial conditions -- IGM structure during galaxy formation
More informationZeldovich pancakes in observational data are cold
Prepared for submission to JCAP Zeldovich pancakes in observational data are cold arxiv:1411.6650v3 [astro-ph.co] 3 May 2017 Thejs Brinckmann, a,b Mikkel Lindholmer, b Steen Hansen, b Martina Falco b,c,d
More informationX-ray and Sunyaev-Zel dovich Effect cluster scaling relations: numerical simulations vs. observations
X-ray and Sunyaev-Zel dovich Effect cluster scaling relations: numerical simulations vs. observations Daisuke Nagai Theoretical Astrophysics, California Institute of Technology, Mail Code 130-33, Pasadena,
More informationPrinceton December 2009 The fine-scale structure of dark matter halos
Princeton December 2009 The fine-scale structure of dark matter halos Simon White Max Planck Institute for Astrophysics The dark matter structure of CDM halos A rich galaxy cluster halo Springel et al
More informationMilky Way Satellite Galaxies with DES
Milky Way Satellite Galaxies with DES Alex Drlica-Wagner kadrlica@fnal.gov! DES Milky Way Working Group Coordinator! January 11, 2015 Milky Way Satellite Galaxies Segue 1 The Milky Way is surrounded by
More informationSpiral Structure. m ( Ω Ω gp ) = n κ. Closed orbits in non-inertial frames can explain the spiral pattern
Spiral Structure In the mid-1960s Lin and Shu proposed that the spiral structure is caused by long-lived quasistatic density waves The density would be higher by about 10% to 20% Stars, dust and gas clouds
More informationMulti-wavelength studies of substructures and inhomogeneities in galaxy clusters
Multi-wavelength studies of substructures and inhomogeneities in galaxy clusters SZE (RX J1347) ΔS X (A3667) Tetsu Kitayama Toho University, Japan Infrared (Coma) 1. How can we study ICM physics with the
More informationConstraints on dark matter annihilation cross section with the Fornax cluster
DM Workshop@UT Austin May 7, 2012 Constraints on dark matter annihilation cross section with the Fornax cluster Shin ichiro Ando University of Amsterdam Ando & Nagai, arxiv:1201.0753 [astro-ph.he] Galaxy
More informationPiTP Summer School 2009
PiTP Summer School 2009 Plan for my lectures Volker Springel Lecture 1 Basics of collisionless dynamics and the N-body approach Lecture 2 Gravitational solvers suitable for collisionless dynamics, parallelization
More informationGalaxies: Structure, Dynamics, and Evolution. Dark Matter Halos and Large Scale Structure
Galaxies: Structure, Dynamics, and Evolution Dark Matter Halos and Large Scale Structure Layout of the Course Feb 5: Review: Galaxies and Cosmology Feb 12: Review: Disk Galaxies and Galaxy Formation Basics
More informationDwarf Galaxies as Cosmological Probes
Dwarf Galaxies as Cosmological Probes Julio F. Navarro The Ursa Minor dwarf spheroidal First Light First Light The Planck Satellite The Cosmological Paradigm The Clustering of Dark Matter The Millennium
More informationResolving the structure and evolution of nearby Galaxy Clusters
Resolving the structure and evolution of nearby Galaxy Clusters Prof. César A. Caretta (Heinz Andernach, Roger Coziol, Josué Trejo-Alonso, Marcel Chow-Martínez, Juan de Anda Suárez, Humberto Santoyo Ruiz,
More informationThe Galaxy Dark Matter Connection. Frank C. van den Bosch (MPIA) Xiaohu Yang & Houjun Mo (UMass)
The Galaxy Dark Matter Connection Frank C. van den Bosch (MPIA) Xiaohu Yang & Houjun Mo (UMass) Introduction PARADIGM: Galaxies live in extended Cold Dark Matter Haloes. QUESTION: What Galaxy lives in
More informationWALLABY. Jeremy Mould WALLABY Science Meeting December 2, 2010
WALLABY Jeremy Mould WALLABY Science Meeting December 2, 2010 Jeremy Mould Seminar: Monash University School of Physics October 7, 2010 Dark Matter Detected in regions where M/L > 100 Outer parts of spiral
More informationAGN feedback and its influence on massive galaxy evolution
AGN feedback and its influence on massive galaxy evolution Darren Croton (University of California Berkeley) Simon White, Volker Springel, et al. (MPA) DEEP2 & AEGIS collaborations (Berkeley & everywhere
More informationVelocity distribution of dark Matter halos: A critical test for the Λ cold dark matter model
UNLV Theses, Dissertations, Professional Papers, and Capstones 5-2010 Velocity distribution of dark Matter halos: A critical test for the Λ cold dark matter model Robert Jo Thompson University of Nevada
More informationGalaxy Formation Now and Then
Galaxy Formation Now and Then Matthias Steinmetz Astrophysikalisches Institut Potsdam 1 Overview The state of galaxy formation now The state of galaxy formation 10 years ago Extragalactic astronomy in
More informationThe build up of the correlation between halo spin and the large-scale structure
Advance Access publication 2017 September 25 doi:10.1093/mnras/stx2466 The build up of the correlation between halo spin and the large-scale structure Peng Wang 1,2 and Xi Kang 1 1 Purple Mountain Observatory,
More informationDetailed energy (mass) budget of the Universe
Detailed energy (mass) budget of the Universe most baryons are in ionized gas outside galaxies Intergalactic baryons Quasar absorption lines zqso=3.18 The Lyα forest as a probe of intergalactic gas The
More informationGalaxy Clusters in Stage 4 and Beyond
Galaxy Clusters in Stage 4 and Beyond (perturbation on a Cosmic Visions West Coast presentation) Adam Mantz (KIPAC) CMB-S4/Future Cosmic Surveys September 21, 2016 Galaxy clusters: what? Galaxy cluster:
More informationThe merger rate of galaxies in the Illustris simulation: a comparison with observations and semi-empirical models
doi:10.1093/mnras/stv264 The merger rate of galaxies in the Illustris simulation: a comparison with observations and semi-empirical models Vicente Rodriguez-Gomez, 1 Shy Genel, 1,2 Mark Vogelsberger, 3
More informationGalaxy Cluster Mergers
Galaxy Cluster Mergers Alexia Schulz Institute for Advanced Study Andrew Wetzel Daniel Holz Mike Warren Talk Overview! Introduction " Why are cluster mergers of interest? " Where will mergers complicate
More informationThe friends-of-friends algorithm: A percolation theory perspective
THE OVERDENSITY AND MASSES OF THE FRIENDS-OF-FRIENDS HALOS AND UNIVERSALITY OF HALO MASS FUNCTION Surhud More 1,2,Andrey V. Kravtsov 2,3,4,Neal Dalal 5,Stefan Gottlöber 6 Draft version February 28, 2011
More informationDark Matter Substructure and their associated Galaxies. Frank C. van den Bosch (MPIA)
Dark Matter Substructure and their associated Galaxies Frank C. van den Bosch (MPIA) Outline PART I: The Subhalo Mass Function (van den Bosch, Tormen & Giocoli, 2005) PART II: Statistical Properties of
More informationThe Milky Way and Near-Field Cosmology
The Milky Way and Near-Field Cosmology Kathryn V Johnston (Columbia University) Collaborators (theorists): James S Bullock (Irvine), Andreea Font (Durham), Brant Robertson (Chicago), Sanjib Sharma (Columbia),
More informationASOHF: a new adaptive spherical overdensity halo finder. S. Planelles and V. Quilis
A&A 519, A94 (2010) DOI: 10.1051/0004-6361/201014214 c ESO 2010 Astronomy & Astrophysics ASOHF: a new adaptive spherical overdensity halo finder S. Planelles and V. Quilis Departament d Astronomia i Astrofísica,
More informationStructure formation in the concordance cosmology
Structure formation in the Universe, Chamonix, May 2007 Structure formation in the concordance cosmology Simon White Max Planck Institute for Astrophysics WMAP3 team WMAP3 team WMAP3 team WMAP3 team In
More informationTesting the cold dark matter model with gravitational lensing
Testing the cold dark matter model with gravitational lensing Priyamvada Natarajan Departments of Astronomy & Physics Yale University In Memoriam: Vera Rubin New Directions in Theoretical Physics, January
More informationWitnessing the onset of environmental quenching at z~1-2. Results from 3D-HST
Witnessing the onset of environmental quenching at z~1-2. Results from 3D-HST Matteo Fossati USM/MPE Munich with D.Wilman, J.T. Mendel, R. Saglia, A. Beifiori, A. Galametz, R. Bender, N.M. Forster Schreiber,
More information